|Title||Composite Supernova Remnants: Home to the Youngest Neutron Stars|
|Author||Prof David Helfand|
|Description||Composite supernova remnants are the relatively small class of remnants which display the expected result of a massive star.s explosion: a central synchrotron nebula powered by a young neutron star, and an expanding shell of emission produced by the stellar ejecta. We propose to observe the two such objects at the extremes of the radio synchrotron core luminosity distribution in order to address such issues as the range of initial pulsar spin periods and magnetic fields. We will also establish their nebular spectral break frequencies which reveal confinement pressures and offer clues as to the pulsars. spin histories. Finally, we will search for emission from surrounding thermal shells which provide an additional constraint on remnant age.|
|Publication||No observations found associated with the current proposal|
|Instrument||EMOS1, EMOS2, EPN, OM, RGS1, RGS2|
|Mission Description||The European Space Agency's (ESA) X-ray Multi-Mirror Mission (XMM-Newton) was launched by an Ariane 504 on December 10th 1999. XMM-Newton is ESA's second cornerstone of the Horizon 2000 Science Programme. It carries 3 high throughput X-ray telescopes with an unprecedented effective area, and an optical monitor, the first flown on a X-ray observatory. The large collecting area and ability to make long uninterrupted exposures provide highly sensitive observations.
Since Earth's atmosphere blocks out all X-rays, only a telescope in space can detect and study celestial X-ray sources. The XMM-Newton mission is helping scientists to solve a number of cosmic mysteries, ranging from the enigmatic black holes to the origins of the Universe itself. Observing time on XMM-Newton is being made available to the scientific community, applying for observational periods on a competitive basis.
|Publisher And Registrant||European Space Agency|
|Credit Guidelines||European Space Agency, 2002-05-19T00:00:00Z, 000421, 17.56_20190403_1200. https://doi.org/10.5270/esa-8xds5xw|